SDSS-V: Pioneering Panoptic Spectroscopy

Kollmeier, Juna A.; Zasowski, Gail; Rix, Hans─Walter; Johns, Matt; Anderson, Scott F.; Drory, Niv; Johnson, Jennifer A.; Pogge, Richard W.; Bird, Jonathan C.; Blanc, Guillermo A.; Brownstein, Joel R.; Crane, Jeffrey D.; Lee, Nathan De; Klaene, Mark A.; Kreckel, Kathryn; MacDonald, Nick; Merloni, A.; Ness, Melissa; O’Brien, Thomas F.; Sánchez-Gallego, José R.; Sayres, Conor; Shen, Ya; Thakar, Ani; Tkachenko, A.; Aerts, C.; Blanton, Michael R.; Eisenstein, Daniel J.; Holtzman, Jon A.; Maoz, Dan; Nandra, K.; Rockosi, Constance M.; Weinberg, David H.; Bovy, Jo; Casey, Andrew R.; Chanamé, Julio; Clerc, N.; Conroy, Charlie; Eracleous, Michael; Gänsicke, B. T.; Hekker, S.; Horne, K.; Kauffmann, Jens; McQuinn, Kristen B. W.; Pellegrini, E.; Schinnerer, E.; Schlafly, Edward F.; Schwope, A. D.; Seibert, Mark; Teske, Johanna; Saders, Jennifer L. van

doi:10.48550/arxiv.1711.03234

Cited by 277 publications

(320 citation statements)

References 33 publications

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“…The formation conditions of halo stars are imprinted in their chemical abundances. Therefore, through observations of the chemical our Galaxy will only continue to grow, with future data releases from the Gaia mission as well as the release of data from current ongoing and planned spectroscopic surveys, including WEAVE (Dalton et al 2014), 4MOST (de Jong et al 2019), DESI (Allende Prieto et al 2020), and SDSS-V (Kollmeier et al 2017). Thanks to these programs, we now have 6D phase space information as well as up to 30+ dimensions of chemical information (e.g., GALAH+ DR3, Buder et al 2021) for millions of stars in the Galaxy, a truly groundbreaking achievement.…”

Section: Introductionmentioning

confidence: 99%

Reading the CARDs: the Imprint of Accretion History in the Chemical Abundances of the Milky Way's Stellar Halo

Cunningham¹,

Sanderson²,

Johnston³

et al. 2021

Preprint

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In the era of large-scale spectroscopic surveys in the Local Group (LG), we can explore using chemical abundances of halo stars to study the star formation and chemical enrichment histories of the dwarf galaxy progenitors of the Milky Way (MW) and M31 stellar halos. In this paper, we investigate using the Chemical Abundance Ratio Distributions (CARDs) of seven stellar halos from the Latte suite of FIRE-2 simulations. We attempt to infer galaxies' assembly histories by modelling the CARDs of the stellar halos of the Latte galaxies as a linear combination of "template" CARDs from disrupted dwarfs, with different stellar masses M and quenching times t 100 . We present a method for constructing these templates using present-day dwarf galaxies. For four of the seven Latte halos studied in this work, we recover the mass spectrum of accreted dwarfs to a precision of < 10%. For the fraction of mass accreted as a function of t 100 , we find residuals of 20-30% for five of the seven simulations. We discuss the failure modes of this method, which arise from the diversity of star formation and chemical enrichment histories dwarf galaxies can take. These failure cases can be robustly identified by the high model residuals. Though the CARDs modeling method does not successfully infer the assembly histories in these cases, the CARDs of these disrupted dwarfs contain signatures of their unusual formation histories. Our results are promising for using CARDs to learn more about the histories of the progenitors of the MW and M31 stellar halos.

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Section: Introductionmentioning

confidence: 99%

Reading the CARDs: the Imprint of Accretion History in the Chemical Abundances of the Milky Way's Stellar Halo

Cunningham¹,

Sanderson²,

Johnston³

et al. 2021

Preprint

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“…By looking at high l-modes in the CνB sky from non-luminous regions, there is a possibility to factor out baryonic effects. Extensive galactic surveys, such as SDSS IV/V, track baryonic matter and can be used to separate CνB anisotropy contibutions at high l-modes according to their baryonic content to provide a more direct handle on the onset of non-linear power effects at low redshift [16].…”

Section: Results and Conclusionmentioning

confidence: 99%

Impact of Warm Dark Matter on the Cosmic Neutrino Background Anisotropies

Tully¹,

Zhang²

2022

Preprint

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The Cosmic Neutrino Background (CνB) anisotropies for massive neutrinos are a unique probe of large-scale structure formation. The redshift-distance measure is completely different for massive neutrinos as compared to electromagnetic radiation. The CνB anisotropies in massive neutrinos grow in response to non-relativistic motion in gravitational potentials seeded by relatively high k-modes. Differences in the early phases of large-scale structure formation in Warm Dark Matter (WDM) versus Cold Dark Matter (CDM) cosmologies have an impact on the magnitude of the CνB anisotropies for contributions to the angular power spectrum that peak at high k-modes. We take the example of WDM consisting of 2 keV sterile neutrinos and show that the CνB anisotropies for 0.05 eV neutrinos drop off at high-l multipole moment in the angular power spectrum relative to CDM. At the same angular scales that one can observe baryonic acoustical oscillations in the CMB, the CνB anisotropies begin to become sensitive to differences in WDM and CDM cosmologies. The precision measurement of high-l multipoles in the CνB neutrino sky map is a potential possibility for the PTOLEMY experiment with thin film targets of spin-polarized atomic tritium superfluid that exhibit significant quantum liquid amplification for non-relativistic relic neutrino capture.

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“…In the next decade, by combining eROSITA with upcoming spectroscopic galaxy surveys (e.g. DESI, SDSS-V, 4MOST: DESI Collaboration et al 2016;Kollmeier et al 2017;de Jong et al 2019;Merloni et al 2019;Finoguenov et al 2019), properties of the CGM and their relation to active galactic nuclei should be unraveled. The eROSITA all-sky survey (eRASS) data cover more than hundred times more extra-galactic sky than eFEDS and therefore offer the opportunity to improve on the analysis presented here.…”

Section: Discussionmentioning

confidence: 99%

The eROSITA Final Equatorial Depth Survey (eFEDS): X-ray emission around star-forming and quiescent galaxies at $0.05

Comparat,

Truong,

Merloni

et al. 2022

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Aims. The circum-galactic medium (CGM) plays an important role in galaxy evolution as the main interface between the star-forming body of galaxies and the surrounding cosmic network of in-and out-flowing matter. In this work, we aim at characterizing the hot phase of the CGM in a large sample of galaxies using recent soft X-ray observations made by SRG/eROSITA. Methods. We stack X-ray events from the 'eROSITA Final Equatorial Depth Survey' (eFEDS) around central galaxies in the 9hr field of the 'GAlaxy and Mass Assembly' (GAMA) survey to construct radially projected X-ray luminosity profiles in the 0.5-2 keV rest frame energy band as a function of their stellar mass and specific star formation rate. We consider samples of quiescent (star-forming) galaxies in the stellar mass range 2 × 10 10 -10 12 M (3 × 10 9 -6 × 10 11 M ). Results. For quiescent galaxies, the X-ray profiles are clearly extended throughout the available mass range; however, the measured profile is likely biased high due to projection effects, as these galaxies tend to live in dense and hot environments. For the most massive star forming samples (≥ 10 11 M ), there is a hint of detection of extended emission. On the other hand, for star-forming galaxies with < 10 11 M the X-ray stacked profiles are compatible with unresolved sources and consistent with the expected emission from faint active galactic nuclei (AGN) and X-ray binaries. We measure for the first time the mean relation between average X-ray luminosity and stellar mass separately for quiescent and star-forming galaxies. We find that the relation is different for the two galaxy populations: high-mass (≥ 10 11 M ) star-forming or quiescent galaxies follow the expected scaling of virialized hot haloes, while lower mass starforming galaxies show a less prominent luminosity and a weaker dependence on stellar mass, consistent with empirical models of the population of weak AGN. When comparing our results with state-of-the art numerical simulations (IllustrisTNG and EAGLE), we find an overall consistency on the average emission on large (> 80 kpc) scales at masses ≥ 10 11 M , but disagreement on the small scales, where brighter than observed compact cores are predicted. The simulations also do not predict the clear differentiation that we observe between quiescent and star-forming galaxies in our samples. Conclusions. This is a stepping stone towards a more profound understanding of the hot phase of the CGM, which holds a key role in the regulation of star formation. Future analysis using eROSITA all-sky survey data, combined with future generation galaxy evolution surveys, shall provide much enhanced quantitative measures and mappings of the circum-galactic medium and its hot phase(s).

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SDSS-V: Pioneering Panoptic Spectroscopy

Cited by 277 publications

References 33 publications

Reading the CARDs: the Imprint of Accretion History in the Chemical Abundances of the Milky Way's Stellar Halo

Reading the CARDs: the Imprint of Accretion History in the Chemical Abundances of the Milky Way's Stellar Halo

Impact of Warm Dark Matter on the Cosmic Neutrino Background Anisotropies

The eROSITA Final Equatorial Depth Survey (eFEDS): X-ray emission around star-forming and quiescent galaxies at $0.05

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